Spitzer IRS Spectral Mapping Of Galactic PDRs: The Atomic-To-Molecular Transition In M17

Details Spitzer IRS Spectral Mapping Of Galactic PDRs: The Atomic-To-Molecular Transition In M17 Spitzer IRS Spectral Mapping Of Galactic PDRs: The Atomic-To-Molecular Transition In M17

May 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...210.1908c&link_type=abstract

American Astronomical Society Meeting 210, #19.08; Bulletin of the American Astronomical Society, Vol. 39, p.120

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We have carried out Spitzer spectral mapping observations of the edge-on Galactic photodissociation region M17, taking advantage of the unprecedented spatial resolution and spectral sensitivity of the IRS. The maps cover the entire atomic-to-molecular transition, from ionized gas in the HII region through the PDR and into the molecular cloud. Using the full IRS high-resolution spectral range from 10-37μm, we have mapped the region in a total of 10 lines - H2 S(0), S(1) and S(2), [Fe II] 26μm, [Si II] 35μm, [S III] 18.7 and 33.5μm, [Ne II] 12.8μm, [Ne III] 15.6μm, [S IV] 10.5μm - as well as in several PAH features. Using the H2 lines, we are able to map the column density, clumpiness, and temperature of warm molecular gas in the PDR. [SiII] and [FeII] emission traces the both the ionized and warm, high-density molecular gas, while the other ionized lines cut off sharply at the ionization front. We compare the observed H2, [SiII] and [FeII] emission with our detailed PDR models in order to constrain the H2 formation rate and photoelectric heating rate and to explore the degree to which FUV photons are able to penetrate into the clumpy molecular cloud. We also present maps of several other Galactic PDRs, NGC2023 and RCW49.
The authors wish to acknowledge NSF grant PHY-0552964 which supports Physics Research Experiences for Undergraduates at San Jose State University, and Spitzer RSAs to the University of Maryland and San Jose State University. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. Support for this work was provided by NASA through awards issued by JPL/Caltech.

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